Nuclear Theory·nucl-th
5 papers—4 primary·1 cross-listed
E. Santopinto🇮🇹 · J. Ferretti🇮🇹
The relativistic interacting quark-diquark model, constructed in the framework of point form dynamics, is extended to strange baryons. The strange and nonstrange baryon spectra are calculated and compared with the experimental data.
Dai-Mei Zhou🇨🇳 · Yu-Liang Yan🇨🇳 · Xing-Long Li🇨🇳 · Xiao-Mei Li🇨🇳 · Bao-Guo Dong🇨🇳 · Xu Cai🇨🇳 · Ben-Hao Sa🇨🇳
The parton and hadron cascade model PACIAE 2.1 (cf. Comput. Phys. Commun.184 (2013) 1476) has been upgraded to the new issue of PACIAE 2.2. By this new issue the lepton-nucleon and lepton-nucleus (inclusive) deep inelastic scatterings can also be investigated. As an example, the PACIAE 2.2 model is enabled to calculate the specific charged hadron multiplicity in the +p and +D semi-inclusive deep-inelastic scattering at 27.6 GeV electron beam energy. The calculated results are well comparing with the corresponding HERMES data. Additionally, the effect of model parameters \alpha and \beta in the Lund string fragmentation function on the multiplicity is studied.
Matthias Drews🇩🇪 · Wolfram Weise🇩🇪
A previous study of nuclear matter in a chiral nucleon-meson model is extended to isospin-asymmetric matter. Fluctuations beyond mean-field approximation are treated in the framework of the functional renormalization group. The nuclear liquid-gas phase transition is investigated in detail as a function of the proton fraction in asymmetric matter. The equations of state at zero temperature of both symmetric nuclear matter and pure neutron matter are found to be in good agreement with realistic many-body computations. We also study the density dependence of the pion mass in the medium. The question of chiral symmetry restoration in neutron matter is addressed; we find a stabilization of the phase with spontaneously broken chiral symmetry once fluctuations are included. Finally, neutron star matter including beta equilibrium is discussed. The model satisfies the constraints imposed by the existence of two-solar-mass neutron stars.
V.B. Kopeliovich (Moscow, INR & Moscow, MIPT)🇷🇺 · G.K. Matushko (Moscow, INR)🇷🇺 · I.K. Potashnikova (Valparaiso, Santa Maria U.)🇨🇱
Analytical explanation of the nuclear glory effect, which is similar to the known optical (atmospheric) glory phenomenon, is presented. It is based on the small phase space method for the multiple interaction processes probability estimates and leads to the characteristic angular dependence of the production cross section in the vicinity of the strictly backward direction, for any number of interactions , either elastic or inelastic. Rigorous proof of this effect is given for the case of the optimal kinematics, as well as for arbitrary polar scattering angles in the case of the light particle rescattering, but the arguments in favor of the backward azimuthal (axial) focusing are quite general and hold for any kind of the multiple interaction processes. Such behaviour of the cross section near the backward direction agrees qualitatively with available data. In the small interval of final angles including the value the angular dependence of the cumulative particle production cross section can have the crater-like (or funnel-like) form. Further studies including, probably, certain numerical calculations, are necessary to clear up this point.
first authorsco-authorsvia INSPIRE